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Front. Astron. Space Sci., 17 October 2017 | https://doi.org/10.3389/fspas.2017.00026

How Quasar Feedback May Shape the Co-evolutionary Paths

  • Physik-Institut, University of Zurich, Zürich, Switzerland

Observations point toward some form of “co-evolutionary sequence,” from dust-enshrouded starbursts to luminous unobscured quasars. Active galactic nucleus (AGN) feedback is generally invoked to expel the obscuring dusty gas in a blow-out event, eventually revealing the hidden central quasar. However, the physical mechanism driving AGN feedback, either due to winds or radiation, remains uncertain and is still a source of much debate. We consider quasar feedback, based on radiation pressure on dust, which directly acts on the obscuring dusty gas. We show that AGN radiative feedback is capable of efficiently removing the obscuring cocoon, and driving powerful outflows on galactic scales, consistent with recent observations. I will discuss how such quasar feedback may provide a natural physical interpretation of the observed evolutionary path, and the physical implications in the broader context of black hole-host galaxy co-evolution.

1. Introduction

Active galactic nuclei (AGN) and nuclear starbursts are observed to be intimately coupled, both fueled by the rapid infall of matter, possibly triggered by galaxy mergers (e.g., Alexander and Hickox, 2012, and references therein). A “co-evolutionary sequence,” starting from dust-obscured starbursts (e.g., ultraluminous infrared galaxies or ULIRG) leading to unobscured optical quasars, has been widely discussed since Sanders et al. (1988). In most evolutionary scenarios, some form of AGN feedback is required to expel the obscuring gas and dust in a short-lived “blow-out” event.

Numerical simulations try to reproduce such an evolutionary sequence, with AGN feedback usually implemented by coupling a fixed fraction of the accretion luminosity to the surrounding medium (Di Matteo et al., 2005; Hopkins et al., 2005). However, the physical mechanism for AGN feedback is not specified, and in particular no explicit connection is made with the dust component (which is the fundamental parameter determining both the source visibility and the spectral energy distribution). On the observational side, there has been renewed interest in the topic, following the discovery of new populations of dust-reddened quasars at high redshifts (close to the peak epoch of both AGN and starburst activities), likely caught in the short-lived blow-out phase (e.g., Banerji et al., 2012, 2015).

Here we propose a physical mechanism that directly makes use of the dust in order to drive AGN feedback, and we briefly discuss how such AGN radiative feedback may naturally explain the observed co-evolutionary path (Ishibashi and Fabian, 2016b).

2. AGN Radiative Feedback: Radiation Pressure on Dust

We consider AGN feedback driven by radiation pressure on dust. The ambient dusty gas is swept up into an outflowing shell, with the corresponding equation of motion given by:

ddt[Msh(r)v]=Lc(1+τIR-e-τUV)-GM(r)Msh(r)r2    (1)

where L is the central luminosity, M(r) is the total mass distribution, Msh(r) is the shell mass, and τIR,UV(r)=κIR,UVMsh(r)4πr2 are the infrared (IR) and ultraviolet (UV) optical depths (Ishibashi and Fabian, 2015; Thompson et al., 2015). We recall that there are 3 distinct physical regimes depending on the optical depth of the medium: optically thick to both IR and UV, optically thick to UV but optically thin to IR (single scattering limit), and optically thin to UV. The associated shell column density is defined as:

Nsh(r)=Msh(r)4πr2mp    (2)

where mp is the proton mass.

By equating the outward force due to radiation pressure to the inward force due to gravity, we can define a critical luminosity, LE, which may be considered as a generalized form of the effective Eddington luminosity. We recall that the effective Eddington luminosity for dusty gas is distinct from the standard Eddington luminosity relevant for ionized gas (Fabian et al., 2006). The corresponding effective Eddington ratio is then given by:

Γ=LLE=Lr2cGM(r)Msh(r)(1+τIR-e-τUV)    (3)

The effective Eddington ratios in the 3 optical depth regimes are respectively given by:

ΓIR=κIRL4πGcM(r);ΓSS=L4πGcmpM(r)Nsh(r);ΓUV=κUVL4πGcM(r)    (4)

Figure 1 shows the effective Eddington ratio as a function of radius, and its dependence on the underlying physical parameters. The effective Eddington ratio basically corresponds to the ratio of the radiative force to the gravitational force, and must exceed unity for an outflowing shell (the standard Eddington limit does not apply here). From Figure 1, we see that an increase in the shell mass leads to a lower Eddington ratio in the single scattering regime (cyan curve); while in the IR-optically thick and UV-optically thin regimes, ΓIR and ΓUV are independent of the shell mass (cf. Equation 4), hence the cyan and black curves overlap at small and large radii. In contrast, enhanced opacities (e.g., due to a higher dust-to-gas ratio) lead to higher Eddington ratios in the IR-optically thick and UV-optically thin regimes (magenta curve); whereas in the single scattering regime, ΓSS is independent of the opacity (cf. Equation 4), and thus the magenta and black curves overlap at intermediate radii. We note that there are two interesting trends in the IR-optically thick regime:

1. The effective Eddington ratio is independent of the shell column density (or shell mass).

2. The effective Eddington ratio directly scales with the opacity, and hence dust-to-gas ratio (as κIRfdg).

FIGURE 1
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Figure 1. Effective Eddington ratio as a function of radius: L = 5 × 1046erg/s, Msh=5×108M, fdg = 1/150 (black, fiducial); L = 5 × 1046erg/s, Msh=1×109M, fdg = 1/150 (cyan); L = 5 × 1046erg/s, Msh=5×108M, fdg = 1/50 (magenta).

The first point implies that even dense material can potentially be disrupted; while the second point implies that the more dusty gas is more easily ejected (Ishibashi and Fabian, 2016b).

3. Dust Obscuration and Blow-Out

In physical terms, dusty gas surrounding the central source absorbs UV radiation and re-emits in the IR band. If the reprocessed IR photons remain trapped in the nuclear regions, the system is effectively in the IR-optically thick regime, where the Eddington ratio is independent of the column density (Equation 4). Such conditions are likely reached in the nuclear regions of ULIRG-like systems, characterized by high densities and high dust-to-gas fractions. This leads to both higher IR optical depth and higher IR-Eddington ratio, which combine to facilitate the blow-out of dusty gas.

In Figure 2 (left panel) we plot the temporal evolution of the shell column density for different values of the central luminosity. We see that the obscuration falls off with time, with the decline being more rapid for brighter sources. In fact, an increase in the luminosity leads to an increase in the effective Eddington ratio in all 3 optical depth regimes, and thus efficient acceleration, and resulting high velocity. The right panel in Figure 2 shows the shell column density as a function of velocity for different values of the dust-to-gas ratio. We observe that a given column is accelerated to higher velocities for larger dust-to-gas fractions: at a given time, the column density is lower for higher dust-to-gas ratios. Indeed, an increase in the dust-to-gas ratio leads to enhanced IR opacity, which in turn leads to a higher Eddington ratio in the IR-optically thick regime. Thus the more dusty gas (which provides much of the obscuration) is preferentially ejected by radiative feedback, and therefore the central quasar has a natural tendency to remove its own obscuring cocoon and reveal itself. We have previously discussed how such AGN-driven dusty outflows may propagate on larger scales beyond the host galaxy, and contribute to the enrichment of the circum-galactic medium (Ishibashi and Fabian, 2016a).

FIGURE 2
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Figure 2. Left: shell column density vs. time for variations in luminosity (Nsh,0=1024cm-2, fdg = 1/150): L = 3 × 1046erg/s (blue), L = 5 × 1046erg/s (black), L = 1 × 1047erg/s (green). Right: shell column density vs. velocity for variations in the dust-to-gas ratio (L = 2 × 1046erg/s, Nsh,0=1024cm-2): fdg = 1/150 (black), fdg = 1/50 (blue), fdg = 1/30 (green). High-luminosity case: L = 1047erg/s, fdg = 1/50 (magenta).

The model results can be compared with observational samples of the recently uncovered populations of dust-reddened quasars and dust-obscured galaxies (Assef et al., 2015; Banerji et al., 2015; Zakamska et al., 2016). These sources are likely observed close to the point of ejecting their obscuring cocoon, and thus may represent the long-sought “sources in transition” (as discussed in Ishibashi and Fabian, 2016b).

4. The Dual Role of Dust: Hiding and Revealing the Central Quasar

The large amounts of gas and dust surrounding the nuclear source provide potential fuel for the central black hole, but that same accreting material is also responsible for significant obscuration. Although AGN feedback is generally invoked to clear the obscuring gas and dust in co-evolutionary scenarios, the actual physical mechanism remains uncertain, with no clear connection to the dust component. In our picture, AGN radiative feedback directly acts on the dusty gas, which forms the obscuring medium. Large amounts of dust imply heavy obscuration, but also powerful feedback, suggesting a causal link between dust obscuration and blow-out. In this scenario, dust plays a dual role: it is responsible for both hiding, but eventually revealing the central quasar.

An important requirement in our model is the presence of dust, since the whole AGN feedback process relies on radiation pressure on dust. The large amount of dust required in order to sustain feedback may be provided by supernovae in the starburst phase. In fact, recent observations indicate that significant quantities of dust can be produced in core-collapse supernovae (Owen and Barlow, 2015; Wesson et al., 2015). Continued star formation in the starburst is beneficial, as it helps keeping the ambient medium dusty, and thus supporting the overall AGN feedback process. Stellar feedback likely disrupts the starburst activity, but the nuclear gas reservoir may also be replenished by re-accretion episodes. Furthermore, we previously suggested that star formation (with subsequent supernova explosions and associated dust release) may be triggered within the AGN feedback-driven outflow itself (Ishibashi and Fabian, 2012). Interestingly, the first direct detection of star formation occurring inside a galactic outflow has now been observationally confirmed (Maiolino et al., 2017), nicely supporting our model predictions. In our framework, AGN feedback and starburst phenomena are intrinsically coupled through the production of dust in supernova explosions, leading to a natural interpretation of the co-evolutionary path.

Author Contributions

The author confirms being the sole contributor of this work and approved it for publication.

Conflict of Interest Statement

The author declares that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.

The reviewer GR and handling Editor declared their shared affiliation.

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Keywords: active galactic nuclei, quasars, feedback, starbursts, galaxies

Citation: Ishibashi W (2017) How Quasar Feedback May Shape the Co-evolutionary Paths. Front. Astron. Space Sci. 4:26. doi: 10.3389/fspas.2017.00026

Received: 24 August 2017; Accepted: 02 October 2017;
Published: 17 October 2017.

Edited by:

Mauro D'Onofrio, Università degli Studi di Padova, Italy

Reviewed by:

Francoise Combes, Observatoire de Paris, France
Giulia Rodighiero, Università degli Studi di Padova, Italy

Copyright © 2017 Ishibashi. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) or licensor are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.

*Correspondence: Wako Ishibashi, wako.ishibashi@physik.uzh.ch